docs(2025): 2025 branch

.placeholder

@@ -1,12 +1,13 @@
 # 2023-12-17 test workflow
 # verified do not run mkdocs gh-deploy it wipes mike
 # ./utils/mike.sh 
-
+#s re on branch 2025 
 # found issue browser is 404 on versions.json updated discussion
 # started tshooting docs to clarify confusions 
 # git push origin 2022
 # git push origin 2023
 # git push origin 2024
 # git push origin main
 # git push origin gh-pages
-# mike deploy --push --update-aliases 2024 latest
+# mike deploy --push --update-aliases 2024 latest
+# mike deploy --update-aliases 2025 latest

backups/index.md

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+---
+tags:
+  - level 1 
+  - level 2 
+---
+
+## buddhism study journals
+
+![ramen](images/ramen.jpeg)
+
+![seated](images/Seated_Buddha.Gandhara.Asian_ArtMuseum.jpg)
+
+- [morning & evening ritual](evening_ritual.md){ .md-button }
+
+- I studied buddhism at home for a few years during covid
+- started a chan meditation class in 2023
+- [x] 2023-24 20 week Chan meditation course [level 1](level_1.md)
+- [x] 2024-25 20 week Chan meditation course [level 2](level_2.md)
+- [ ] 2025 level 3 40 week course [level 3](level_3.md)
+- [ ] 2027-31 sutra study 80 week course
+
+## command line apps for memorizing sutras
+
+<iframe width="859" height="531" src="https://www.youtube.com/embed/vllKiMq-q3M" title="memorization: python click app for memorizing the heart sutra (or anything)" frameborder="0" allow="accelerometer; autoplay; clipboard-write; encrypted-media; gyroscope; picture-in-picture; web-share" referrerpolicy="strict-origin-when-cross-origin" allowfullscreen></iframe>
+
+## research notes on buddhism
+
+[diamond sutra: the mind seal of prajna wisdom audiobook](https://www.ctworld.org.tw/Buddhist%20e-Books/Audio/Book007/index.html){ .md-button }
+[heart sutra study](https://www.ctworld.org.tw/Buddhist%20e-Books/Books05/index.html){ .md-button }
+[seven round compassion contemplation](seven_full.md){ .md-button }
+[books](books.md){ .md-button }
+
+<iframe width="1120" height="700" src="https://www.youtube.com/embed/J3dLt9TaAnw" title="buddhism homepage" frameborder="0" allow="accelerometer; autoplay; clipboard-write; encrypted-media; gyroscope; picture-in-picture; web-share" allowfullscreen></iframe>
+
+[TAGS]

backups/particles_energy.md

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+---
+tags:
+  - summary 
+---
+# summary
+
+## particles
+
+### 1. **The Fate of Atoms:**
+
+- Over vast timescales, the energy levels of atoms could be disrupted by processes in the universe, causing them to lose their electrons:
+  - **Proton Decay (Hypothetical):** If protons are not stable (some theories predict they might decay after \(10^{31}\) to \(10^{34}\) years), atoms would disintegrate entirely.
+  - **Ionization by Background Radiation:** In a sufficiently energetic environment (like near stars or in a superheated cosmic state), electrons could be stripped from atoms.
+  - **Expansion of the Universe:** The cooling and spreading of matter in an ever-expanding universe would reduce interactions that allow atoms to retain bound electrons.
+
+---
+
+### 2. **High Entropy Universe:**
+
+- **Entropy** is a measure of disorder or the number of microstates in a system. Over time, the universe tends toward a state of maximum entropy:
+  - Stars will burn out and stop forming (Stellar Era ends in about \(10^{14}\) years).
+  - Black holes will dominate and slowly evaporate through Hawking radiation over \(10^{100}\) years.
+  - Remaining matter will decay into subatomic particles, leaving a "soup" of electrons, photons, and neutrinos.
+
+---
+
+### 3. **Heat Death of the Universe:**
+
+- The ultimate fate of the universe may be **heat death** or **thermal equilibrium**, where:
+  - All energy differences are dissipated.
+  - No structures (atoms, stars, galaxies) can exist.
+  - Only low-energy particles (like photons and leptons) remain, spread uniformly across space.
+  - This is a high-entropy state because no usable energy or complex structures are left.
+
+---
+
+### 4. **How Does This Relate to Atoms?**
+
+- In the process of reaching thermal equilibrium:
+  - Atoms may lose their electrons and dissociate entirely.
+  - The remaining protons, neutrons, and electrons might decay or be subsumed into other forms of matter (if protons decay, for example).
+
+---
+
+### 5. **Final State:**
+
+The "soup" you refer to would consist of:
+
+- Diffuse particles (e.g., photons, neutrinos, and possibly some stable remnants like dark matter).
+- No organized structures, just a high-entropy, low-energy fog.
+
+This scenario aligns with what physicists call the **Big Freeze**, a possible end-state of the universe. Would you like to explore this further?
+
+## energy
+
+on a **cosmic timescale**, most forms of energy in the universe are gradually dissipating, converting, or "discharging" in processes governed by the laws of **thermodynamics** and **cosmic evolution**. Here's how each type of energy evolves or dissipates over time:
+
+---
+
+### 1. **Kinetic Energy**
+
+- **Dissipation:** Motion slows down as systems lose energy through friction, collisions, or radiation. For example:
+  - Orbiting celestial bodies lose energy through **gravitational radiation** (e.g., binary systems emitting gravitational waves).
+  - Gas clouds and particles lose kinetic energy as they cool and settle.
+
+---
+
+### 2. **Potential Energy**
+
+- **Dissipation:** Potential energy is often converted to kinetic or radiant energy:
+  - **Gravitational Potential Energy:** Released as heat or light when objects fall into gravitational wells (e.g., stars forming, black holes accreting matter). Over time, fewer systems remain to collapse.
+  - Eventually, in a far future where no significant structures exist, potential energy becomes irrelevant.
+
+---
+
+### 3. **Thermal Energy**
+
+- **Dissipation:** Heat spreads as systems reach **thermal equilibrium**:
+  - Stars radiate heat and eventually cool to white dwarfs, neutron stars, or black holes.
+  - The interstellar medium cools over billions of years as galaxies stop forming stars.
+  - Cosmic Microwave Background (CMB) radiation cools with the universe's expansion, heading toward absolute zero.
+
+---
+
+### 4. **Radiant Energy**
+
+- **Dissipation:** Photons (light and other electromagnetic waves) lose energy due to:
+  - **Redshift:** The expansion of the universe stretches wavelengths, reducing photon energy (e.g., CMB photons have cooled from the Big Bang's intense heat to 2.7 K today).
+  - Over time, photons spread thinly across space, becoming nearly undetectable.
+
+---
+
+### 5. **Nuclear Energy**
+
+- **Dissipation:** Nuclear reactions diminish as fuel depletes:
+  - Stars exhaust their nuclear fuel, transitioning to white dwarfs or black holes.
+  - Free protons in the universe may decay (if proton decay occurs, estimated at \(10^{31}\)-\(10^{34}\) years).
+  - Fusion and fission processes cease when no usable nuclei remain.
+
+---
+
+### 6. **Chemical Energy**
+
+- **Dissipation:** Chemical processes become irrelevant in a cooling universe:
+  - Molecular reactions require energy differentials, which diminish as the universe reaches thermal equilibrium.
+  - Eventually, even stable molecules and chemical bonds may be disrupted by high-entropy environments.
+
+---
+
+### 7. **Electromagnetic Energy**
+
+- **Dissipation:** Electromagnetic fields weaken:
+  - Magnetic fields decay as their sources (stars, planets) cool and die.
+  - Electric currents in astrophysical systems slow as the universe becomes more diffuse and less conductive.
+
+---
+
+### 8. **Dark Energy**
+
+- **Persistence:** Dark energy is a unique case:
+  - It doesn't seem to dissipate but rather dominates over time, driving the accelerated expansion of the universe.
+  - This expansion contributes to the isolation of energy systems and speeds the universe's journey to high entropy.
+
+---
+
+### 9. **Gravitational Energy**
+
+- **Dissipation:** Gravitational energy converts into heat, waves, or gets trapped:
+  - Gravitational waves carry energy away from merging systems like black holes or neutron stars.
+  - Over time, as galaxies and clusters drift apart, gravity weakens due to the expanding universe.
+
+---
+
+### 10. **Mass Energy (E=mc²)**
+
+- **Dissipation:** Mass energy gradually converts into radiation or disintegrates:
+  - Particle-antiparticle annihilation transforms mass into radiant energy.
+  - Proton decay (if it occurs) converts mass into lighter particles and radiation.
+
+---
+
+### 11. **Quantum Energy**
+
+- **Persistence and fluctuation:**
+  - Quantum fluctuations (vacuum energy) persist even in empty space.
+  - Zero-point energy (the minimum quantum energy) is unlikely to discharge entirely.
+
+---
+
+### 12. **Cosmological Energy**
+
+- **Decay or persistence:** Energy tied to phenomena like inflation or cosmic strings dissipates in early-universe processes. Dark energy may remain indefinitely.
+
+---
+
+### 13. **Dark Matter Energy**
+
+- **Persistence:** Dark matter seems to decay slowly or not at all over cosmic timescales. However, its role diminishes as structures drift apart due to dark energy.
+
+---
+
+### 14. **Mechanical Energy**
+
+- **Dissipation:** Celestial mechanical energy (e.g., orbits) gradually converts to heat or gravitational waves until systems disintegrate or stabilize.
+
+---
+
+### 15. **Acoustic Energy**
+
+- **Dissipation:** Sound waves require a medium and dissipate as gas and matter in the universe cool and thin out. Large-scale cosmic acoustic waves (like baryon acoustic oscillations) are "frozen" into the structure of galaxies.
+
+---
+
+### 16. **Vacuum Energy**
+
+- **Persistence:** Vacuum energy is theorized to remain constant, possibly driving eternal expansion.
+
+---
+
+### **Heat Death and Energy Dissipation**
+
+The ultimate fate of all energy discharge is the **heat death of the universe**:
+
+- All usable energy (differences in energy forms) becomes evenly distributed.
+- The universe reaches maximum entropy—a state where no work or structure is possible.
+- Only a diffuse soup of low-energy photons, neutrinos, and other particles remains, expanding forever or stagnating in a frozen void.
+
+Would you like to dive deeper into a specific type of energy or its cosmic evolution?
+